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As part of Herschel's key programme ”Gas in Protoplanetary Systems” (GASPS), we have analyzed far-IR (60-190 μm) spectra of protoplanetary discs around 76 T Tauri stars locatedin Taurus in different evolutionary states (Class I down to Class III), 27 show jet/outflow activity. We derived fluxes of all detected atomic and molecular lines - [OI], [CII], CO, H_2O and OH - to produce a complete and consistent FIR lines catalogue. Outflow sources are found to have the richest spectra and highest line fluxes, while non-outflow sources are rather poor in lines. We find correlations between several emission lines which suggests a common origin. To verify whether the line emission is associated with the protoplanetary disc or shocks, we compared the observed line fluxes and their ratios with disc and shock models. We find that just from an observational perspective, the outflow rather than the disc dominates the emission at early evolutionary stages (Class I/II).

We present optical imaging and long slit spectroscopic observations of nine luminous type\ud 2 active galactic nuclei (AGN) within the redshift range 0.3

We present optical imaging and long slit spectroscopic observations of 9 luminous type 2 AGNs within the redshift range 0.3, Accepted for publication in MNRAS. 17 pages

La hipertrofia de labios menores es una patología poco frecuente, que puede presentarse a cualquier edad, si bien es más frecuente su detección durante la pubertad. Se trata de una variante anatómica cuya etiología aún es incierta, que se describe como el tejido protuberante localizado tras los labios mayores. Actualmente no existen criterios clínicos objetivos consensuados para definirla. Se trata de una entidad de carácter benigno cuya sintomatología es muy variada, abarcando desde síntomas leves tales como irritación local o problemas con la higiene local, hasta infecciones crónicas, dolor al caminar, dispareunia o problemas psicológicos y estéticos. Una sencilla exploración física desde la consulta pediátrica de Atención Primaria permitirá reconocer fácilmente esta patología, y su posterior derivación al Servicio de Ginecología para su corrección quirúrgica. Labia minora hypertrophy is an uncommon condition that can occur at any age, but is most common during puberty. It is an anatomical variant of uncertain etiology, described as protruding tissue behind labia minora. Currently there are no agreed clinical criteria to define this condition. It is a benign entity whose symptoms are very varied, ranging from mild symptoms such as local irritation or problems with local hygiene, to chronic infections, pain when walking, dyspareunia or psychological and aesthetic problems. A simple physical examination from a pediatric primary care will easily recognize this disease for the subsequent referral to the gynecology department for surgical correction.

We present a 2D study of the internal extinction on (sub)kiloparsec scales of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7), based on near-infrared Paα, Brδ, and Brγ line ratios, obtained with VLT-SINFONI integral-field spectroscopy (IFS). The 2D extinction (AV) distributions of the objects, map regions of ~ 3 × 3 kpc (LIRGs) and ~ 12 × 12 kpc (ULIRGs), with average angular resolutions (FWHM) of ~0.2 kpc and ~0.9 kpc, respectively. The individual AV galaxy distributions indicate a very clumpy dust structure already on sub-kiloparsec scales, with values (per spaxel) ranging from AV ~ 1 to 20 mag in LIRGs, and from AV ~ 2 to 15 mag in ULIRGs. As a class, the median values of the distributions are AV = 5.3 mag and AV = 6.5 mag for the LIRG and ULIRG subsamples, respectively. In ~70% of the objects, the extinction peaks at the nucleus with values ranging from AV ~ 3 to 17 mag. Within each galaxy, the AV radial profile shows a mild decrement in LIRGs within the inner 2 kpc radius, while the same radial variation is not detected in ULIRGs, likely because of the lower linear scale resolution of the observations at the distance of ULIRGs. We evaluated the effects of the galaxy distance in the measurements of the extinction as a function of the linear scale (in kpc) of the spaxel (i.e. due to the limited angular resolution of the observations). If the distribution of the gas/dust and star-forming regions in local LIRGs (63 Mpc, 40 pc/spaxel on average) is the same for galaxies at greater distances, the observed median AV values based on emission line ratios would be a factor ~0.8 lower at the average distance of our ULIRG sample (328 Mpc, 0.2 kpc/spaxel), and a factor ~0.67 for galaxies located at distances of more than 800 Mpc (0.4 kpc/spaxel). This distance effect would have implications for deriving the intrinsic extinction in high-z star-forming galaxies and for subsequent properties such as star formation rate, star formation surface density, and KS- law, based on Hα line fluxes. If local LIRGs are analogues of the main-sequence star-forming galaxies at cosmological distances, the extinction values (AV) derived from the observed emission lines in these high-z sources would need to be increased by a factor 1.4 on average.

We present Hubble Space Telescope/Wide Field Camera 3 narrow-band imaging of the Hα emission in a sample of eight gravitationally lensed galaxies at z = 1-1.5. The magnification caused by the foreground clusters enables us to obtain a median source plane spatial resolution of 360pc, as well as providing magnifications in flux ranging from ~10× to ~50×. This enables us to identify resolved star-forming Hii regions at this epoch and therefore study their Hα luminosity distributions for comparisons with equivalent samples at z ~ 2 and in the local Universe. We find evolution in the both luminosity and surface brightness of Hii regions with redshift. The distribution of clump properties can be quantified with an Hii region luminosity function, which can be fit by a power law with an exponential break at some cut-off, and we find that the cut-off evolves with redshift. We therefore conclude that 'clumpy' galaxies are seen at high redshift because of the evolution of the cut-off mass; the galaxies themselves follow similar scaling relations to those at z = 0, but their Hii regions are larger and brighter and thus appear as clumps which dominate the morphology of the galaxy. A simple theoretical argument based on gas collapsing on scales of the Jeans mass in a marginally unstable disc shows that the clumpy morphologies of high-z galaxies are driven by the competing effects of higher gas fractions causing perturbations on larger scales, partially compensated by higher epicyclic frequencies which stabilize the disc., RCL acknowledges a studentship from STFC, RGB and IS are supported by STFC and IS further acknowledges a Leverhulme Senior Fellowship. AMS acknowledges an STFC Advanced Fellowship, and JR is supported by the Marie Curie Career Integration Grant 294074. HE gratefully acknowledges financial support from STScI grants GO-09722, GO-10491, GO10875 and GO-12166. This work is based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for Program number 12197 and Program number 11678 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555

We present an atlas of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7) covering the luminosity range log(LIR/L⊙) = 11.1−12.4. The atlas is based on near-infrared H (1.45−1.85 μm) and K-band (1.95−2.45 μm) VLT-SINFONI integral field spectroscopy (IFS). The atlas presents the ionised, partially ionised, and warm molecular gas two-dimensional flux distributions and kinematics over an FoV of ~3 × 3 kpc (LIRGs) and ~12 × 12 kpc (ULIRGs) and with average linear resolutions of ~0.2 kpc and ~0.9 kpc, respectively. The different phases of the gas show a wide morphological variety with the nucleus as the brightest Brγ source for ~33% of the LIRGs and ~71% of the ULIRGs, whereas all the LIRGs and ULIRGs have their maximum H2 emission in their nuclear regions. In LIRGs, the ionised gas distribution is dominated by the emission from the star-forming rings or giant HII regions in the spiral arms. The Brγ and [FeII] line at 1.644 μm trace the same structures, although the emission peaks at different locations in some of the objects, and the [FeII] seems to be more extended and diffuse. The ULIRG subsample is at larger distances and contains mainly pre-coalescence interacting systems. Although the peaks of the molecular gas emission and the continuum coincide in ~71% of the ULIRGs, regions with intense Paα (Brγ) emission tracing luminous star-forming regions located at distances of 2−4 kpc away from the nucleus are also detected, usually associated with secondary nuclei or tidal tails. LIRGs have mean observed (i.e. uncorrected for internal extinction) SFR surface densities of about 0.4 to 0.9 M⊙ yr-1 kpc-2 over large areas (4−9 kpc2) with peaks of about 2−2.5 M⊙ yr-1 kpc-2 in the smaller regions (0.16 kpc2) associated with the nucleus of the galaxy or the brightest Brγ region. ULIRGs do have similar average SFR surface densities for the integrated emitting regions of ~0.4 M⊙ yr-1 kpc-2 in somewhat larger areas (100−200 kpc2) and for the Paα peak (~2 M⊙ yr-1 kpc-2 in 4 kpc2). The observed gas kinematics in LIRGs is primarily due to rotational motions around the centre of the galaxy, although local deviations associated with radial flows and/or regions of higher velocity dispersions are present. The ionised and molecular gas share the same kinematics (velocity field and velocity dispersion) to first order, showing slight differences in the velocity amplitudes (peak-to-peak) in some cases, whereas the average velocity dispersions are compatible within uncertainties. As expected, the kinematics of the ULIRG subsample is more complex, owing to the interacting nature of the objects of the sample.

Spatially resolved near-IR and X-ray imaging of the central region of the Luminous Infrared Galaxy NGC 5135 is presented. The kinematical signatures of strong outflows are detected in the [FeII]1.64 ��m emission line in a compact region at 0.9 kpc from the nucleus. The derived mechanical energy release is consistent with a supernova rate of 0.05-0.1 yr$^{-1}$. The apex of the outflowing gas spatially coincides with the strongest [FeII] emission peak and with the dominant component of the extranuclear hard X-ray emission. All these features provide evidence for a plausible direct physical link between supernova-driven outflows and the hard X-ray emitting gas in a LIRG. This result is consistent with model predictions of starbursts concentrated in small volumes and with high thermalization efficiencies. A single high-mass X-ray binary (HMXB) as the major source of the hard X-ray emission although not favoured, cannot be ruled out. Outside the AGN, the hard X-ray emission in NGC 5135 appears to be dominated by the hot ISM produced by supernova explosions in a compact star-forming region, and not by the emission due to HMXB. If this scenario is common to U/LIRGs, the hard X-rays would only trace the most compact (< 100 pc) regions with high supernova and star formation densities, therefore a lower limit to their integrated star formation. The SFR derived in NGC 5135 based on its hard X-ray luminosity is a factor of two and four lower than the values obtained from the 24 ��m and soft X-ray luminosities, respectively., Accepted for Publication in ApJ, 18 pages, 2 figures

Aims. We study the analogy between local U/LIRGs and high-z massive SFGs by comparing basic H�� structural characteristics, such as size, and luminosity (and SFR) surface density, in an homogeneous way (i.e. same tracer and size definition, similar physical scales). Methods. We use Integral Field Spectroscopy based H�� emission maps for a representative sample of 54 local U/LIRGs (66 galaxies). From this initial sample we select 26 objects with H�� luminosities (L(H��)) similar to those of massive (i.e. M\ast \sim 10^10 M\odot or larger) SFGs at z \sim 2, and observed on similar physical scales. Results. The sizes of the H�� emitting region in the sample of local U/LIRGs span a large range, with r1/2(H��) from 0.2 to 7 kpc. However, about 2/3 of local U/LIRGs with Lir > 10^11.4 L\odot have compact H�� emission (i.e. r1/2 < 2 kpc). The comparison sample of local U/LIRGs also shows a higher fraction (59%) of objects with compact H�� emission than the high-z sample (25%). This gives further support to the idea that for this luminosity range the size of the star forming region is a distinctive factor between local and distant galaxies of similar SF rates. However, when using H�� as a tracer for both local and high-z samples, the differences are smaller than the ones recently reported using a variety of other tracers. Despite of the higher fraction of galaxies with compact H�� emission, a sizable group (\sim 1/3) of local U/LIRGs are large (i.e. r1/2 > 2 kpc). These are systems showing pre-coalescence merger activity and they are indistinguishable from the massive high-z SFGs galaxies in terms of their H�� sizes, and luminosity and SFR surface densities., Accepted for publication in A&A. (!5 pages, 7 figures, 2 tables)

We have analyzed the spatially integrated kinematic properties of the ionized gas within the inner r~2). While the quiescent gas shows small or null velocity shifts relative to the systemic velocity, the highly perturbed gas trends to show larger shifts which, moreover, are blueshifts in general. Within a given object, the most perturbed gas trends to have the largest blueshift as well. All together support that the perturbed gas, which is responsible for the blue asymmetries of the line profiles, is outflowing. Although some bias affects the sample, we argue that ionized gas outflows are a common phenomenon in optically selected type 2 quasars at 0.3< z < 0.6., Comment: Accepted for publication in MNRAS. 12 pages, 18 figures

By observing the local luminous infrared galaxy NGC5135 with the near-IR IFU spectrograph SINFONI (ESO-VLT), we report an approx. 600 pc (in projection) AGN outflow traced by [SiVI]1.96mum emission. This is the largest outflow traced by a coronal line ever reported. Its large spatial scale suggests that shocks, in addition to AGN continuum emission, are needed to locally produce [SiVI] emission. We also show, for the first time, clear kinematical evidence of the AGN-outflow vs. ISM interaction through variations in the 2D velocity fields of different gas phases. Such local perturbations in the kinematics clearly match the outflow structure. We use the [FeII]1.64mum emission, a supernovae tracer, to estimate the supernovae rate in different star-forming knots (approx. 250 pc across) within the central 2.3 kpc of NGC5135. The estimated supernovae rates go from 0.02 to 0.08 yr^{-1} being in excellent agreement with predictions from 6 cm radio emission in the same areas., Comment: 6 pages, 3 figures. To appear in A.S.P. Conference Series, "Galaxy Evolution: Infrared to Millimeter Wavelength Perspective", 25-29 October 2010, Guilin, China

NIRSpec will be the first slit-based astronomical multi-object spectrograph to fly in space, and is designed to provide spectra of faint objects over the near-infrared 1.0 - 5.0 micron wavelength range at spectral resolutions of R=100, R=1000 and R=2700. The instrument's all-reflective wide-field optics, together with its novel MEMS-based programmable micro-shutter array slit selection device and its large format low-noise HgCdTe detector arrays, combine to allow simultaneous observations of >100 objects within a 3.4 x 3.5 arcmin field of view with unprecedented sensitivity. A selectable 3 x 3 arcsec Integral Field Unit and five fixed slits are also available for detailed spectroscopic studies of single objects. NIRSpec is being built for the European Space Agency (ESA) by EADS Astrium as part of ESA's contribution to the JWST mission. The NIRSpec micro-shutter and detector arrays are provided by NASA/GSFC.

We describe the current status of the HARMONI instrument design, which will form the basis for the first-light integral field spectrograph on the European Extremely Large Telescope. We review the phase A design, and highlight current on-going work to evolve the design in-line changing telescope requirements and lessons learned during the Phase A work. We also outline the key science drivers for the instrument, and describe briefly the requirements for the laser tomographic adaptive optics system which is expected to feed HARMONI.

We describe the observations and preliminary results of the gas-phase analysis based on two ongoing, wide-field Integral Field Spectroscopy (IFS) surveys: the PPAK IFS Nearby Galaxies Survey (PINGS), targeting disc galaxies; and the VIMOS-IFU observations of low-z (Ultra)Luminous Infrared Galaxies (U-LIRGs), the local counterpart of massive, dusty high-z star-forming galaxies. We describe how these observations are allowing to discover and characterise abundance differentials between galactic substructures and differences depending on the morphologically/dynamically distinct types of objects, which in turn will allow us to interpret the gas-phase abundances of analogue high-z systems., Comment: 8 pages, to appear in Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society held on September 13-17, 2010, in Madrid, Spain

Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society, September 13 - 17, 2010, Madrid,Spain, A statistical analysis of almost 3000 star forming regions (knots) in a representative sample of 32 (U)LIRGs has been performed by means of high angular resolution ACS/HST B and I images. We present the results of the photometric characterization of these star forming regions as a function of the infrared luminosity of the systems (we have split the sample in three luminosity bins) and the interaction phase (four interaction phases have been defined). Properties such as sizes, colors and luminosities are compared with those of clusters observed in less luminous interacting galaxies and the state-of-the-art models of major mergers, This work has been supported by the Spanish Ministry of Education and Science, under grant BES2007-16198, projects ESP2005-01480 and ESP2007-65475-C02-01. The author also thanks the centre at CEA-Saclay for their hospitality during his stay while part of this work was done.

Ante la anunciada reforma de la Ley Orgánica de libertad religiosa, este trabajo pretende poner de manifiesto cuál debe ser el fundamento de la proyectada reforma y cuáles son los aspectos sobre los que debería incidir. A tales efectos se pro- ponen unas líneas de actuación referidas al sujeto individual y colectivo de la libertad religiosa, orientadas a alcanzar mayores cotas de libertad en el ejercicio de este derecho fundamental. In light of the announced reform of the Organic Law on Religious Freedom in Spain, the purpose of this paper is to highlight the grounds on which the reform process should rest and the main points it should address. Different of proposals are made regarding both the individual and collective subject of religious freedom, in order to achieve the best possible legal framework for the free exercise of religion.

Science Perspectives for 3D Spectroscopy, 10-14 October 2005, Garching, Germany

We provide an overview of the most important calibration aspects of the NICMOS instrument on board of HST. We describe the performance of the instrument after the installation of the NICMOS Cooling System, and show that the behavior of the instrument has become very stable and predictable. We detail the improvements made to the NICMOS pipeline and outline plans for future developments. The derivation of the absolute photometric zero-point calibration is described in detail. Finally, we describe and quantify a newly discovered count-rate dependent non-linearity in the NICMOS cameras. This new non-linearity is distinctly different from the total count dependent non-linearity that is well known for near-infrared detectors. We show that the non-linearity has a power law behavior, with pixels with high system, or vice versa, pixels with low count rate detecting slightly less than expected. The effect has a wavelength dependence with observations at the shortest wavelengths being the most affected (~0.05-0.1 mag per dex flux change at ~1 micron, 0.03 mag per dex at 1.6 micron)., Comment: 12 pages, 10 figures. More information on the newly discovered NICMOS count-rate dependent non-linearity and how to correct for it can be found at http://www.stsci.edu/hst/nicmos/performance/anomalies/nonlinearity.html